Fig. 5: Saturation of the no-cosines flow

<p>Left: Volume rendering of the magnetic field and velocity flow in the experiment with Rem = 200 and Re = 200 during saturation. Isosurfaces of regions of low magnetic field and flow (light structures) and local maxima (dark). The lines are magnetic field lines (dark) and stream lines (light). Right: Strong magnetic field (light) and vorticity structures (dark) in the experiment Rem = 200 and Re = 400 during saturation. Field lines traced from weak magnetic field (left side of the box) are stretched and pile up in twisted sheets around strong vortex tubes (to the right).</p>
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<p>From the paper "On the Saturation of Astrophysical Dynamos: Numerical Experiments with the No-Cosines Flow" by S. B. F. DorchV. Archontis.</p>
<p>Published in: Solar Physics October 2004.</p>
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